24 Sep 2013 DaMaSC 2 Feng 1 DARK MATTER AND ITS PARTICLE PROPERTIES Jonathan Feng, UC Irvine Dark Matter in Southern California (DaMaSC 2) Keck Institute for Space Studies, Caltech

24 Sep 2013 DaMaSC 2 Feng 2 DARK MATTER CANDIDATES

24 Sep 2013 DaMaSC 2 Feng 3 OUTLINE WIMPs ̶ Symmetric and Asymmetric ̶ Direct Detection ̶ Indirect Detection ̶ Colliders ̶ Complementarity Axions Warm Dark Matter –Sterile Neutrinos –SuperWIMPs Self-Interacting Dark Matter ̶ Hidden Sector Dark Matter

24 Sep 2013 DaMaSC 2 Feng 4 00 10       0 The relation between  X and annihilation strength is wonderfully simple: m X ~ 100 GeV, g X ~ 0.6   X ~ 0.1 Remarkable coincidence: particle physics independently predicts particles with the right density to be dark matter X X q q _ THE WIMP MIRACLE

24 Sep 2013 DaMaSC 2 Feng 5 STABILITY This all assumes the WIMP is stable How natural is this? New Particle States Standard Model Particles Stable

24 Sep 2013 DaMaSC 2 Feng 6 LEP’S COSMOLOGICAL LEGACY Simple solution: impose a discrete parity, so all interactions require pairs of new particles. This also makes the lightest new particle stable: LEP constraints ↔ Discrete Symmetry ↔ Stability The result: new, stable particles at the weak scale are predicted in many models, motivates DM with m DM ~ 5 GeV Cheng, Low (2003); Wudka (2003) new particle Higgs Gauge Hierarchy requires SM new particle Precision EW excludes

24 Sep 2013 DaMaSC 2 Feng 7 ASYMMETRIC DARK MATTER The SM matter relic density was not generated by freeze-out, but by an asymmetry If the dark matter relic density was generated in a similar way n DM ~ n B ↓ m DM / m B ~  DM /  B ~ 5 Asymmetric DM motivates “light WIMPs” with m DM ~ 5 GeV Baryons Baryons 10 9 Anti- Baryons 10 9 Anti- Baryons

24 Sep 2013 DaMaSC 2 Feng 8 DIRECT DETECTION Dark matter elastically scatters off nuclei Nuclear recoils detected by phonons, scintillation, ionization, …, … e,  DM Attisha

24 Sep 2013 DaMaSC 2 Feng 9 CURRENT STATUS AND FUTURE PROSPECTS background: Billard, Strigari, Figueroa-Feliciano (2013) Asymmetric n DM ~ n B

24 Sep 2013 DaMaSC 2 Feng 10 INDIRECT DETECTION Dark matter may pair annihilate in our galactic neighborhood to Photons Neutrinos Positrons Antiprotons Antideuterons The relic density provides a target annihilation cross section  A v  ~ 3 x cm 3 /s

24 Sep 2013 DaMaSC 2 Feng 11 AN EXAMPLE: PHOTONS Current: Veritas, Fermi-LAT, HAWC, Magic, HESS, … Future: Cerenkov Telescope Array (CTA)

24 Sep 2013 DaMaSC 2 Feng 12 INDIRECT DETECTION: PHOTONS Fermi-LAT has excluded a light WIMP with the target annihilation cross section for certain annihilation channels CTA extends the reach to WIMP masses ~ 10 TeV Funk (2013)

24 Sep 2013 DaMaSC 2 Feng 13 DARK MATTER AT COLLIDERS Full Models (e.g., pMSSM Supersymmetry) DM Effective Theories (Bare Bones Dark Matter) X q X q Mono-whatever , j, W, Z Cascades

24 Sep 2013 DaMaSC 2 Feng 14 Before a signal: Different experimental approaches are sensitive to different dark matter candidates with different characteristics, and provide us with different types of information – complementarity! DARK MATTER COMPLEMENTARITY Mass measurement for m > 500 GeV? Lifetime: s  s? Asymmetric DM? Detailed particle properties? After a signal: we are trying to identify a quarter of the Universe: need high standards to claim discovery and follow-up studies to measure properties

24 Sep 2013 DaMaSC 2 Feng 15 COMPLEMENTARITY: FULL MODELS pMSSM 19-parameter scan of SUSY parameter space Different SUSY models are probed by different experiments Cahill-Rowley et al. (2013)

24 Sep 2013 DaMaSC 2 Feng 16 Strongly motivated by the strong CP problem Current bound from electric dipole moments is Motivates introduction of the axion field, which couples to two photons AXIONS 4m

24 Sep 2013 DaMaSC 2 Feng 17 Many production mechanisms, but all yield cold dark matter Parameter space constrained by –Supernova cooling, etc. –Relic density –Direct detection constraints AXION PROPERTIES Favored mass:  eV to meV ADMX is projected to cover the first of these three decades in its first year of operations, and the second decade over the following two years

24 Sep 2013 DaMaSC 2 Feng 18 STERILE NEUTRINOS Strongly motivated by the fact that neutrinos have mass No SM gauge interactions, but they mix with the active neutrinos Correct relic density for ~keV masses

24 Sep 2013 DaMaSC 2 Feng 19 STERILE NEUTRINO PROPERTIES Decays may be detected as X-ray lines May be warm dark matter, depending on mass and production mechanism Abazajian, Koushiappas (2006) Kusenko (2009)

24 Sep 2013 DaMaSC 2 Feng 20 Dark matter could be in a hidden “dark sector,” with no SM couplings; this is viable and perhaps even natural, since all solid evidence for DM is gravitational However, a priori, it’s a bit unsatisfying –Missing the particle physics motivations of many popular DM candidates –Too much model-building freedom, lack of predictivity –Makes no use of the WIMP miracle HIDDEN SECTOR DARK MATTER SM

24 Sep 2013 DaMaSC 2 Feng 21 WIMPless Miracle: Consider hidden sectors in SUSY models. In many models, m X ~ g X 2, which leaves the relic density invariant Restores –Particle physics motivations –Structure, predictivity –The miracle: SUSY hidden sectors automatically have DM with the right  Self-interactions: Observations vs. simulations motivate self-interacting DM with  T /m ~ 0.1–1 cm 2 /g (or barn/GeV) WIMPs WIMPless DM MOTIVATIONS FOR HIDDEN DARK MATTER Feng, Kumar (2008); Feng, Tu, Yu (2009) Rocha et al. (2012), Peter et al. (2012); Vogelsberger et al. (2012); Zavala et al. (2012)

24 Sep 2013 DaMaSC 2 Feng 22 SELF-INTERACTING DM FROM SU(N) HIDDEN SECTOR WIMPless miracle requires weak interactions, self-interactions require strong interactions A natural possibility to consider is a non-Abelian hidden sector with weak coupling at high scales and early times, and strong coupling at low scales now (cf. QCD) Boddy, Feng, Kaplinghat, Tait (2013) Feng, Kaplinghat, Yu (2010); Tulin, Yu, Zurek (2013) Feng, Shadmi (2011)

24 Sep 2013 DaMaSC 2 Feng 23 SELF-INTERACTING DM FROM SU(N) HIDDEN SECTOR An extremely simple possibility: AMSB with a pure SU(N) hidden sector (just hidden gluons and gluinos) ~1-10 TeV gluinos freezeout with the correct relic density At  ~ 10 MeV, (gg̃) and (gg) bound states form (gg̃) dark matter strongly self-interacts through (gg) exchange Boddy, Feng, Kaplinghat, Tait (2013)

24 Sep 2013 DaMaSC 2 Feng 24 SUMMARY Many interesting dark matter candidates Vanilla WIMPs are still very well motivated, as are other cold dark matter candidates, such as axions But there are also well-motivated warm dark matter candidates and self-interacting dark matter candidates Astrophysics may motivate specific candidates and provides unique probes of particle properties